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mathjax"> Micromegas with GEM preamplification for enhanced energy threshold in low-background gaseous time projection chambers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Castel%2C+J">J. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">D. D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">J. Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+A">A. Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/physics?searchtype=author&query=Porr%C3%B3n%2C+J">J. Porr贸n</a>, <a href="/search/physics?searchtype=author&query=Puyuelo%2C+M+J">M. J. Puyuelo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.19864v1-abstract-short" style="display: inline;"> Background: we develop the concept of a Micromegas (MICRO-MEsh GAseous Structure) readout plane with an additional GEM (Gas Electron Multiplier) preamplification stage placed a few mm above it, to increase the maximum effective gain of the combined readout. We implement it and test it in realistic conditions for its application to low-background dark matter searches like the TREX-DM experiment. Me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19864v1-abstract-full').style.display = 'inline'; document.getElementById('2412.19864v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.19864v1-abstract-full" style="display: none;"> Background: we develop the concept of a Micromegas (MICRO-MEsh GAseous Structure) readout plane with an additional GEM (Gas Electron Multiplier) preamplification stage placed a few mm above it, to increase the maximum effective gain of the combined readout. We implement it and test it in realistic conditions for its application to low-background dark matter searches like the TREX-DM experiment. Methods: for this, we use a Micromegas of microbulk type, built with radiopure materials. A small test chamber allowing for systematic scanning of voltages and pressures is used. In addition, a TREX-DM full-scale set-up has also been built and tested, featuring a replica of the fully-patterned TREX-DM microbulk readout. Results: we report on GEM effective extra gain factors of about 90, 50 and 20 in 1, 4 and 10 bar of Ar-1%iC$_{4}$H$_{10}$. Conclusions: the results here obtained show promise to lower the threshold of the experiment down to 50 eV$_{ee}$, corresponding to substantially enhanced sensitivity to low-mass WIMPs (Weakly Interacting Massive Particles). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19864v1-abstract-full').style.display = 'none'; document.getElementById('2412.19864v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, corresponding authors: 脫scar P茅rez (oscarperlaz@unizar.es), H茅ctor Mirallas (mirallas@unizar.es)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.13915">arXiv:2411.13915</a> <span> [<a href="https://arxiv.org/pdf/2411.13915">pdf</a>, <a href="https://arxiv.org/format/2411.13915">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> An accurate solar axions ray-tracing response of BabyIAXO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ahyoune%2C+S">S. Ahyoune</a>, <a href="/search/physics?searchtype=author&query=Altenmueller%2C+K">K. Altenmueller</a>, <a href="/search/physics?searchtype=author&query=Antolin%2C+I">I. Antolin</a>, <a href="/search/physics?searchtype=author&query=Basso%2C+S">S. Basso</a>, <a href="/search/physics?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/physics?searchtype=author&query=Candon%2C+F+R">F. R. Candon</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/physics?searchtype=author&query=Chouhan%2C+D">D. Chouhan</a>, <a href="/search/physics?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/physics?searchtype=author&query=Cervera-Cortes%2C+M">M. Cervera-Cortes</a>, <a href="/search/physics?searchtype=author&query=Chernov%2C+V">V. Chernov</a>, <a href="/search/physics?searchtype=author&query=Civitani%2C+M+M">M. M. Civitani</a>, <a href="/search/physics?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/physics?searchtype=author&query=Costa%2C+E">E. Costa</a>, <a href="/search/physics?searchtype=author&query=Cotroneo%2C+V">V. Cotroneo</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Derbin%2C+A">A. Derbin</a>, <a href="/search/physics?searchtype=author&query=Desch%2C+K">K. Desch</a>, <a href="/search/physics?searchtype=author&query=Diaz-Martin%2C+M+C">M. C. Diaz-Martin</a>, <a href="/search/physics?searchtype=author&query=Diaz-Morcillo%2C+A">A. Diaz-Morcillo</a>, <a href="/search/physics?searchtype=author&query=Diez-Ibanez%2C+D">D. Diez-Ibanez</a>, <a href="/search/physics?searchtype=author&query=Pardos%2C+C+D">C. Diez Pardos</a>, <a href="/search/physics?searchtype=author&query=Dinter%2C+M">M. Dinter</a>, <a href="/search/physics?searchtype=author&query=Doebrich%2C+B">B. Doebrich</a> , et al. (102 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.13915v2-abstract-short" style="display: inline;"> BabyIAXO is the intermediate stage of the International Axion Observatory (IAXO) to be hosted at DESY. Its primary goal is the detection of solar axions following the axion helioscope technique. Axions are converted into photons in a large magnet that is pointing to the sun. The resulting X-rays are focused by appropriate X-ray optics and detected by sensitive low-background detectors placed at th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13915v2-abstract-full').style.display = 'inline'; document.getElementById('2411.13915v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.13915v2-abstract-full" style="display: none;"> BabyIAXO is the intermediate stage of the International Axion Observatory (IAXO) to be hosted at DESY. Its primary goal is the detection of solar axions following the axion helioscope technique. Axions are converted into photons in a large magnet that is pointing to the sun. The resulting X-rays are focused by appropriate X-ray optics and detected by sensitive low-background detectors placed at the focal spot. The aim of this article is to provide an accurate quantitative description of the different components (such as the magnet, optics, and X-ray detectors) involved in the detection of axions. Our efforts have focused on developing robust and integrated software tools to model these helioscope components, enabling future assessments of modifications or upgrades to any part of the IAXO axion helioscope and evaluating the potential impact on the experiment's sensitivity. In this manuscript, we demonstrate the application of these tools by presenting a precise signal calculation and response analysis of BabyIAXO's sensitivity to the axion-photon coupling. Though focusing on the Primakoff solar flux component, our virtual helioscope model can be used to test different production mechanisms, allowing for direct comparisons within a unified framework. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13915v2-abstract-full').style.display = 'none'; document.getElementById('2411.13915v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 18 figures, 4 tables, Submitted to JHEP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.09727">arXiv:2404.09727</a> <span> [<a href="https://arxiv.org/pdf/2404.09727">pdf</a>, <a href="https://arxiv.org/format/2404.09727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Using Micromegas detectors for direct dark matter searches: challenges and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Altenmueller%2C+K">K. Altenmueller</a>, <a href="/search/physics?searchtype=author&query=Antolin%2C+.">. Antolin</a>, <a href="/search/physics?searchtype=author&query=Calvet%2C+D">D. Calvet</a>, <a href="/search/physics?searchtype=author&query=Candon%2C+F+R">F. R. Candon</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J">J. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebrian%2C+S">S. Cebrian</a>, <a href="/search/physics?searchtype=author&query=Cogollos%2C+C">C. Cogollos</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=Ibanez%2C+D+D">D. Diez Ibanez</a>, <a href="/search/physics?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/physics?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/physics?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/physics?searchtype=author&query=Gomez%2C+H">H. Gomez</a>, <a href="/search/physics?searchtype=author&query=Gu%2C+Y">Y. Gu</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+A">A. Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G Irastorza</a>, <a href="/search/physics?searchtype=author&query=Luzon%2C+G">G. Luzon</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Solorzano%2C+A+O">A. Ortiz de Solorzano</a>, <a href="/search/physics?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/physics?searchtype=author&query=Perez%2C+O">O. Perez</a>, <a href="/search/physics?searchtype=author&query=Picatoste%2C+E">E. Picatoste</a>, <a href="/search/physics?searchtype=author&query=Porron%2C+J">J. Porron</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.09727v1-abstract-short" style="display: inline;"> Gas time projection chambers (TPCs) with Micromegas pixelated readouts are being used in dark matter searches and other rare event searches, due to their potential in terms of low background levels, energy and spatial resolution, gain, and operational stability. Moreover, these detectors can provide precious features,such as topological information, allowing for event directionality and powerful s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09727v1-abstract-full').style.display = 'inline'; document.getElementById('2404.09727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09727v1-abstract-full" style="display: none;"> Gas time projection chambers (TPCs) with Micromegas pixelated readouts are being used in dark matter searches and other rare event searches, due to their potential in terms of low background levels, energy and spatial resolution, gain, and operational stability. Moreover, these detectors can provide precious features,such as topological information, allowing for event directionality and powerful signal-background discrimination. The Micromegas technology of the microbulk type is particularly suited to low-background applications and is being exploited by detectors for CAST and IAXO (solar axions) and TREX-DM (low-mass WIMPs) experiments. Challenges for the future include reducing intrinsic background levels, reaching lower energy detection levels, and technical issues such as robustness of detector, new design choices, novel gas mixtures and operation points, scaling up to larger detector sizes, handling large readout granularity, etc. We report on the status and prospects of the development ongoing in the context of IAXO and TREX-DM experiments, pointing to promising perspectives for the use of Micromegas detectors in directdark matter searches <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09727v1-abstract-full').style.display = 'none'; document.getElementById('2404.09727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.06316">arXiv:2403.06316</a> <span> [<a href="https://arxiv.org/pdf/2403.06316">pdf</a>, <a href="https://arxiv.org/format/2403.06316">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Background discrimination with a Micromegas detector prototype and veto system for BabyIAXO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Altenm%C3%BCller%2C+K">K. Altenm眉ller</a>, <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">J. F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">S. Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">T. Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Iba%C3%B1ez%2C+D">D. D铆ez-Iba帽ez</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+A">A. Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Ferrer-Ribas%2C+E">E. Ferrer-Ribas</a>, <a href="/search/physics?searchtype=author&query=Galan%2C+J">J. Galan</a>, <a href="/search/physics?searchtype=author&query=Galindo%2C+J">J. Galindo</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Giganon%2C+A">A. Giganon</a>, <a href="/search/physics?searchtype=author&query=Goblin%2C+C">C. Goblin</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">I. G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Loiseau%2C+C">C. Loiseau</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">G. Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Navick%2C+X+F">X. F. Navick</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">C. Margalejo</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">H. Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">L. Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">A. Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=Papaevangelou%2C+T">T. Papaevangelou</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">O. P茅rez</a>, <a href="/search/physics?searchtype=author&query=Quintana%2C+A">A. Quintana</a>, <a href="/search/physics?searchtype=author&query=Ruz%2C+J">J. Ruz</a>, <a href="/search/physics?searchtype=author&query=Vogel%2C+J+K">J. K. Vogel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.06316v1-abstract-short" style="display: inline;"> In this paper we present measurements performed with a Micromegas X-ray detector setup. The detector is a prototype in the context of the BabyIAXO helioscope, which is under construction to search for an emission of the hypothetical axion particle from the sun. An important component of such a helioscope is a low background X-ray detector with a high efficiency in the 1-10 keV energy range. The go… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.06316v1-abstract-full').style.display = 'inline'; document.getElementById('2403.06316v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.06316v1-abstract-full" style="display: none;"> In this paper we present measurements performed with a Micromegas X-ray detector setup. The detector is a prototype in the context of the BabyIAXO helioscope, which is under construction to search for an emission of the hypothetical axion particle from the sun. An important component of such a helioscope is a low background X-ray detector with a high efficiency in the 1-10 keV energy range. The goal of the measurement was to study techniques for background discrimination. In addition to common techniques we used a multi-layer veto system designed to tag cosmogenic neutron background. Over an effective time of 52 days, a background level of $8.6 \times 10^{-7}\,\text{counts keV}^{-1}\,\text{cm}^{-2} \, \text{s}^{-1}$ was reached in a laboratory at above ground level. This is the lowest background level achieved at surface level. In this paper we present the experimental setup, show simulations of the neutron-induced background, and demonstrate the process to identify background signals in the data. Finally, prospects to reach lower background levels down to $10^{-7} \, \text{counts keV}^{-1} \, \text{cm}^{-2} \, \text{s}^{-1}$ will be discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.06316v1-abstract-full').style.display = 'none'; document.getElementById('2403.06316v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.12622">arXiv:2312.12622</a> <span> [<a href="https://arxiv.org/pdf/2312.12622">pdf</a>, <a href="https://arxiv.org/format/2312.12622">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Searching for WIMPs with TREX-DM: achievements and challenges </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Castel%2C+J+F">Juan F. Castel</a>, <a href="/search/physics?searchtype=author&query=Cebri%C3%A1n%2C+S">Susana Cebri谩n</a>, <a href="/search/physics?searchtype=author&query=Dafni%2C+T">Theopisti Dafni</a>, <a href="/search/physics?searchtype=author&query=D%C3%ADez-Ib%C3%A1%C3%B1ez%2C+D">David D铆ez-Ib谩帽ez</a>, <a href="/search/physics?searchtype=author&query=Ezquerro%2C+%C3%81">脕lvaro Ezquerro</a>, <a href="/search/physics?searchtype=author&query=Gal%C3%A1n%2C+J">Javier Gal谩n</a>, <a href="/search/physics?searchtype=author&query=Garc%C3%ADa%2C+J+A">Juan Antonio Garc铆a</a>, <a href="/search/physics?searchtype=author&query=Irastorza%2C+I+G">Igor G. Irastorza</a>, <a href="/search/physics?searchtype=author&query=Jim%C3%A9nez%2C+M">Mar铆a Jim茅nez</a>, <a href="/search/physics?searchtype=author&query=Luz%C3%B3n%2C+G">Gloria Luz贸n</a>, <a href="/search/physics?searchtype=author&query=Margalejo%2C+C">Cristina Margalejo</a>, <a href="/search/physics?searchtype=author&query=de+Mira%2C+%C3%81">脕ngel de Mira</a>, <a href="/search/physics?searchtype=author&query=Mirallas%2C+H">Hector Mirallas</a>, <a href="/search/physics?searchtype=author&query=Obis%2C+L">Luis Obis</a>, <a href="/search/physics?searchtype=author&query=de+Sol%C3%B3rzano%2C+A+O">Alfonso Ortiz de Sol贸rzano</a>, <a href="/search/physics?searchtype=author&query=P%C3%A9rez%2C+O">Oscar P茅rez</a>, <a href="/search/physics?searchtype=author&query=Ruz%2C+J">Jaime Ruz</a>, <a href="/search/physics?searchtype=author&query=Vogel%2C+J">Julia Vogel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.12622v1-abstract-short" style="display: inline;"> The TREX-DM detector, a low background chamber with microbulk Micromegas readout, was commissioned in the underground laboratory of Canfranc (LSC) in 2018. Since then, data taking campaigns have been carried out with Argon and Neon mixtures, at different pressures from 1 to 4 bar. By achieving a low energy threshold of 1 keV$_{ee}$ and a background level of 80 counts keV$^{-1}$ Kg$^{-1}$ day… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12622v1-abstract-full').style.display = 'inline'; document.getElementById('2312.12622v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.12622v1-abstract-full" style="display: none;"> The TREX-DM detector, a low background chamber with microbulk Micromegas readout, was commissioned in the underground laboratory of Canfranc (LSC) in 2018. Since then, data taking campaigns have been carried out with Argon and Neon mixtures, at different pressures from 1 to 4 bar. By achieving a low energy threshold of 1 keV$_{ee}$ and a background level of 80 counts keV$^{-1}$ Kg$^{-1}$ day$^{-1}$ in the region from 1 to 7 keV$_{ee}$, the experiment demonstrates its potential to search for low-mass WIMPs. Two of the most important challenges currently faced are the reduction of both, background level and energy threshold. With respect to the energy threshold, recently a new readout plane is being developed, based on the combination of Micromegas and GEM technologies, aiming to have a pre-amplification stage that would permit very low energy thresholds, close to the single-electron ionization energy. With respect to the background reduction, apart from studies to identify and minimize contamination population, a high sensitivity alpha detector is being developed in order to allow a proper material selection for the TREX-DM detector components. Both challenges, together with the optimization of the gas mixture used as target for the WIMP detection, will take TREX-DM to explore regions of WIMP's mass below 1 GeV c$^{-2}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12622v1-abstract-full').style.display = 'none'; document.getElementById('2312.12622v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">LIDINE 2023: LIght Detection In Noble Elements</span> </p> </li> </ol> <div class="is-hidden-tablet"> <!-- feedback for mobile only --> <span class="help" style="display: inline-block;"><a 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